Speaker
Description
In the standard disk galaxy formation model, the sizes of galactic disks are tightly related to the spin parameters of their dark matter haloes. The model has been wildly adopted by various semi--analytic galaxy formation models which have been extremely successful to interpret a large body of observational data. However, the size-$\lambda$ correlation was rarely seen in most modern hydrodynamical simulations of galaxy formation. We found galactic sizes correlate with spin parameters of their dark matter haloes in the simulations developed by the IllustrisTNG collaborations, albeit the relation does not always agree with prediction of MMW98 model overall stellar mass range we examined. Further, We explored how different AURIGA and APOSTLE sub-grid models, especially for stellar feedback, influence angular momentum evolution of disc galaxies, by comparing two suits of zoom-in simulations with identical initial conditions. Our results demonstrate that the gas recycling process has a significant impact on the evolution of angular momentum after the gas fall into the galaxy. Specifically, we find that the higher baryon recycling efficiency in the AURIGA simulation leads to galaxies with higher angular momentum magnitude and alignment than in the APOSTLE simulation.
